Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +07° 3142

Djurašević, G.; Yılmaz, M.; Baştürk, Özgür; Kílíçoǧlu, T.; Latković, O.; Çalışkan, Şeyma

doi:10.1051/0004-6361/201014895

Cited by 26 publications

(7 citation statements)

References 36 publications

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“…The effective temperature was computed to be in the range 5200 K -5300 K, making it a K2V-K0V system. The deduced period of ASAS 105331 − 7424.7 was 0.4825 ± 0.0002, which is consistent with the measured periods of other close binaries such as QX and RW Com [18]. Thus, the derived linear ephemeris equation for ASAS 110609 − 2045.3 is given by:…”

Section: Asas 105331 − 74247supporting

confidence: 83%

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Photometric Study of Three Short-Period Eclipsing Binaries from the ASAS Catalogue

Obu¹,

Okeke²

2013

IJAA

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We carried out high-precision photometric observations of three eclipsing ultrashort-period contact binaries (USPCBs). Theoretical models were fitted to the light-curves by means of the Wilson-Devinney code. The solutions suggest that the three targets have evolved to a contact phase. The photometric results are as follows: a) 1SWASP J030749.87−365201.7, q = 0.439 ± 0.003, f = 0.0±3.6 %; b) 1SWASP J213252.93−441822.6, q = 0.560±0.003, f = 14.2±1.9 %; c) 1SWASP J200059.78+054408.9, q = 0.436 ± 0.008, f = 58.4 ± 1.8 %. The light curves show O'Connell effects, which can be modeled by assumed cool spots. The cool spots models are strongly supported by the night-tonight variations in the I-band light curves of 1SWASP J030749.87−365201.7. For a comparative study, we collected the whole set of 28 well-studied USPCBs with P < 0.24 day. Thus, we found that most of them (17 of 28) are in shallow contact (i.e. fill-out factors f < 20 %). Only 4 USPCBs have deep fill-out factors (i.e. f > 50 %). Generally, contact binaries with deep fill-out factors are going to merge, but it

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Section: Asas 105331 − 74247supporting

confidence: 83%

“…The computed value of the angle of inclination of the system is 80˚ ± 1 to the line of sight. We also established that ASAS 110609 − 2045.3 has a mass ratio of about 0.5, a value that is consistent with other W Uma-type binaries such as RW Com and BD + 07˚ 3142 [18]. The system showed evidence of a third Table 3.…”

Section: Asas 110609-20453supporting

confidence: 83%

Photometric Study of Three Short-Period Eclipsing Binaries from the ASAS Catalogue

Obu¹,

Okeke²

2013

IJAA

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“…While the Galactic bulge systems do not have their spectroscopy done so far, many of the ASAS ones from Lee (2015) have their parameters published (e.g. Dimitrov et al 2014;Djurašević et al 2011;He lminiak et al 2009He lminiak et al , 2015aRatajczak et al 2013Ratajczak et al , 2016Różyczka et al 2013). …”

Section: Comparison With the Tres Resultsmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the results of our spectroscopic observations of eight detached eclipsing binaries (DEBs), selected from the Kepler Eclipsing Binary Catalog. Radial velocities (RVs) were calculated from high resolution spectra obtained with the HIDES spectrograph, attached to the 1.88-m telescope of the Okayama Astrophysical Observatory, and were used to characterize the targets in combination with the Kepler light curves. For each binary we obtained a full set of orbital and physical parameters, reaching precision below 3% in masses and radii for 5 pairs. By comparing our results with theoretical models, we assess the distance, age and evolutionary status of the researched objects. We also study eclipse timing variations of selected objects, and identify a new system with a γDor pulsator. Two systems are triples, and show lines coming from three components. In one case the motion of the outer star and the perturbation in the RVs of the inner binary are clearly visible and periodical, which allows us to directly calculate the mass of the third star, and inclination of the outer orbit. In the second case we only see a clear motion of the tertiary, and investigate two scenarios: that it is a linear trend coming from the orbital motion around the inner binary, and that it is caused by a planetary mass companion. When possible, we also compare our results with the literature, and conclude that only by combining photometry with RVs it is possible to obtain correct physical parameters of both components of a DEB.

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“…To date, only two other LMDEBs are known to be in a similar configuration: BD ‐22 5866, which is a system with a K7+K7 eclipsing pair and an M1+M2 non‐eclipsing binary (Shkolnik et al ), and YY Gem, which is the faintest member of a sextuple system, composed of three spectroscopic binaries, Castor A, B and C (α Gem ABC; Vinter Hansen, Neubauer & Roosen‐Raad ; Kron ; Bopp ). There are also a few examples of LMDEBs known to have a single additional companion, such as LP 133‐373 (Vaccaro et al ), HIP 96515 (Huélamo et al ), MR Del (Pribulla et al ; Djurašević et al ), NLTT 41135 (Irwin et al ), ASAS‐08 (Montes et al ; Hełminiak & Konacki ) or the triply eclipsing KOI‐126 (Carter et al ). Such systems not only allow more rigid constraints on the evolutionary models than in the cases of ‘lonely’ eclipsing binaries, but they also play an important role in testing star‐formation theories, stellar population codes and dynamical interactions in multiple stellar systems.…”

Section: Discussionmentioning

confidence: 99%

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

Hełminiak

Konacki

Rozyczka

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present the orbital and physical parameters of a newly discovered low‐mass detached eclipsing binary from the All‐Sky Automated Survey (ASAS) data base: ASAS J011328–3821.1 A, which is a member of a visual binary system with the secondary component separated by about 1.4 arcsec. The radial velocities have been calculated from the high‐resolution spectra obtained with the 1.9‐m Radcliffe telescope/Grating Instrument for Radiation Analysis with a Fibre‐Fed Echelle (GIRAFFE) spectrograph, the 3.9‐m Anglo‐Australian Telescope (AAT)/University College London Echelle Spectrograph (UCLES) and the 3.0‐m Shane telescope/Hamilton Spectrograph (HamSpec) on the basis of the todcor technique and the positions of the Hα emission lines. For the analysis, we have used V‐ and I‐band photometry obtained with the 1.0‐m Elizabeth telescope and the 0.41‐m Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT), supplemented with the publicly available ASAS light curve of the system. We have found that ASAS J011328–3821.1 A is composed of two late‐type dwarfs, which have masses of M1 = 0.612 ± 0.030 M⊙ and M2 = 0.445 ± 0.019 M⊙ and radii of R1 = 0.596 ± 0.020 R⊙ and R2 = 0.445 ± 0.024 R⊙. Both show a substantial level of activity, which manifests in strong Hα and Hβ emission and the presence of cool spots. The influence of the third light on the eclipsing pair properties has also been evaluated and the photometric properties of component B have been derived. A comparison with several popular stellar evolution models shows that the system is on its main‐sequence evolution stage and that it is probably more metal‐rich than the Sun. We have also found several clues to suggest that component B itself is a binary composed of two nearly identical ∼0.5‐M⊙ stars.

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Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +07° 3142

Cited by 26 publications

References 36 publications

Photometric Study of Three Short-Period Eclipsing Binaries from the ASAS Catalogue

Photometric Study of Three Short-Period Eclipsing Binaries from the ASAS Catalogue

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

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